Tvashtar awakening detected in April 2006 with OSIRIS at the W.M. Keck Observatory

Laver, Conor; Pater, Imke de; Marchis, Franck

doi:10.1016/j.icarus.2007.06.022

Cited by 21 publications

(6 citation statements)

References 29 publications

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“…We also note that the photometry of OSIRIS data at the 20 mas platescale is not perfect, due to a loss of flux into the PSF halo. Although to first approximation our calibration procedure has taken this into account, we adopt a 15% uncertainty in our absolute flux calibration, based on previous OSIRIS observations (Laver et al 2007). Our results are shown in Figs.…”

Section: Observationsmentioning

confidence: 99%

“…We corrected both primary and secondary object spectra for telluric absorption in Earth's atmosphere, and photometrically calibrated them in a manner similar to that described by Laver et al (2007), using observed spectra of the stars HD77281 (type A2) and HD111133 (type A0), both 2MASS catalog stars (see Table 1). The telluric correction was determined by comparing the spectra of the stars to the calibrated spectra from stellar atmosphere models.…”

Section: Observationsmentioning

confidence: 99%

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Component-resolved near-infrared spectra of the (22) Kalliope system

Laver

Pater

Marchis

et al. 2009

Icarus

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We observed (22) Kalliope and its companion Linus with the integral-field spectrograph OSIRIS, which is coupled to the adaptive optics system at the W.M. Keck 2 telescope on March 25 2008. We present, for the first time, component-resolved spectra acquired simultaneously in each of the Zbb (1-1.18µm), Jbb (1.18-1.42µm), Hbb (1.47-1.80µm), and Kbb (1.97-2.38µm) bands. The spectra of the two bodies are remarkably similar and imply that both bodies were formed at the same time from the same material; such as via incomplete re-accretion after a major impact on the precursor body.

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Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Component-resolved near-infrared spectra of the (22) Kalliope system

Laver

Pater

Marchis

et al. 2009

Icarus

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“…Hyperspectral data (>100 discrete wavelengths) of volcanic activity on the Jovian moon Io have been obtained by the Voyager and Galileo spacecraft at extremely low spatial resolutions [ Carr , 1986; Davies et al , 2001; Lopes et al , 2001; Davies , 2003]. Voyager thermal infrared (TIR) data coupled with the Near Infrared Mapping Spectrometer (NIMS) have been used to determine eruption style from thermal signatures at many volcanoes on Io [e.g., Laver et al , 2007; Davies , 2007]. However, the surface temperature distribution of an active lava flow is typically heterogeneous at the scale of even the smallest image pixel [e.g., Flynn and Mouginis‐Mark , 1994].…”

Section: Introductionmentioning

confidence: 99%

Spatial variations in lava flow field thermal structure and effusion rate derived from very high spatial resolution hyperspectral (MIVIS) data

Lombardo¹,

Harris²,

Calvari³

et al. 2009

J. Geophys. Res.

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[1] High spatial resolution hyperspectral measurements of volcanic thermal anomalies allow for an unconstrained solution of a two-component thermal model. This can be used for identification of lava flow emplacement style and the calculation of lava flow heat and volume flux. The multispectral infrared and visible imaging spectrometer (MIVIS) is an airborne sensor equipped with 72 bands in the short infrared range and 10 bands in the thermal infrared region of the spectrum. We used MIVIS acquired for Mount Etna (Italy) during the July-August 2001 eruption to solve the dual band equations in an unconstrained fashion using three bands of unsaturated data. Our results suggest a complex thermal structure for Etnean lava flows. This is characterized by a downflow transition from a lightly crusted active channel to a more heavily crusted distal section, both surrounded by zones of stagnant cooling flow where exposed molten material is absent and maximum temperatures are thus lower. The total flow field effusion rate obtained for 29 July 2001 (0700 local time) of 8-16 m 3 /s is in excellent agreement with that obtained from ground-based measurements and Advanced Very High Resolution Radiometer data. Flow-by-flow effusion rates obtained from the MIVIS data vary depending on whether the vent is linked to the central conduit or the dyke that was injected from greater depth, as well as vent elevation, with lower elevation vents experiencing higher effusion rates.

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“…On each night an A-type star with J, H, and K magnitudes from 2MASS was used to correct for telluric absorption, instrument spectral response, and for photometry as described by Laver et al (2007). A second-order photometric correction was performed using 113 IRTF spectra (Brown, M. E., private communication).…”

Section: Observationsmentioning

confidence: 99%

Observations of the global haze redistribution on Titan from 2006 to 2015 with OSIRIS at Keck

Ádámkovics

Pater

2017

Icarus

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We observed Titan with the OH Suppressing InfraRed Imaging Spectrograph (OSIRIS) at the W. M. Keck observatory from 2006 through 2015 using adaptive optics. The sunlight scattered by atmospheric haze was spatially resolved in the 2.0 µm (K) band window, and the spectra were analyzed with a radiative transfer model to determine the vertical (altitude) and meridional (latitudinal) variation in the haze distribution over this time period. This study complements recent work by Karkoschka (2016) in the season of observations, in the time span and sampling interval, in wavelength coverage and spectral resolution, as well as in the radiative transfer methodology and analysis. We observe the largest meridional gradient in haze opacity above 20 km toward the northern hemisphere in January 2010. Individual observations can show significant deviations from a relatively smooth linear gradient in haze across the entire disk. The variation in haze below 20 km is rarely well-described by a simple model and there is a systematically smaller amount of haze opacity retrieved from the Equator to 10 • S when observing the disk with a sub-observer longitude near 150 • W. This correlation with longitude suggests one of the following; a localized decrease in haze scattering, a localized increase in gas opacity, or a systematic overestimate of the surface albedo in this region.

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Tvashtar awakening detected in April 2006 with OSIRIS at the W.M. Keck Observatory

Cited by 21 publications

References 29 publications

Component-resolved near-infrared spectra of the (22) Kalliope system

Component-resolved near-infrared spectra of the (22) Kalliope system

Spatial variations in lava flow field thermal structure and effusion rate derived from very high spatial resolution hyperspectral (MIVIS) data

Observations of the global haze redistribution on Titan from 2006 to 2015 with OSIRIS at Keck

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